Mariah G. Macdonald, Darin Ragozzine, Daniel C. Fabrycky, Eric B. Ford, Matthew J. Holman, Howard T. Isaacson, Jack J. Lissauer, Eric D. Lopez, Tsevi Mazeh, Leslie Rogers, Jason F. Rowe, Jason H. Steffen, Guillermo Torres

Research output: Contribution to journalArticlepeer-review

92 Scopus citations


Kepler has discovered hundreds of systems with multiple transiting exoplanets which hold tremendous potential both individually and collectively for understanding the formation and evolution of planetary systems. Many of these systems consist of multiple small planets with periods less than ∼50 days known as Systems with Tightly spaced Inner Planets, or STIPs. One especially intriguing STIP, Kepler-80 (KOI-500), contains five transiting planets: f, d, e, b, and c with periods of 1.0, 3.1, 4.6, 7.1, and 9.5 days, respectively. We provide measurements of transit times and a transit timing variation (TTV) dynamical analysis. We find that TTVs cannot reliably detect eccentricities for this system, though mass estimates are not affected. Restricting the eccentricity to a reasonable range, we infer masses for the outer four planets (d, e, b, and c) to be 6.75-0.51 +0.69,4.13-0.95 +0.81 , 6.93-0.70 +1.05, 6.74-0.86 +1.23 and Earth masses, respectively. The similar masses but different radii are consistent with terrestrial compositions for d and e and ∼2% H/He envelopes for b and c. We confirm that the outer four planets are in a rare dynamical configuration with four interconnected three-body resonances that are librating with few degree amplitudes. We present a formation model that can reproduce the observed configuration by starting with a multi-resonant chain and introducing dissipation. Overall, the information-rich Kepler-80 planets provide an important perspective into exoplanetary systems.

Original languageEnglish (US)
Article number105
JournalAstronomical Journal
Issue number4
StatePublished - Oct 2016

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science


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